scholarly journals A method for determining the radius of an open cluster from stellar proper motions

2018 ◽  
Vol 475 (3) ◽  
pp. 4122-4132 ◽  
Author(s):  
Néstor Sánchez ◽  
Emilio J Alfaro ◽  
Fátima López-Martínez
Keyword(s):  
Open Cluster ◽  
Proper Motions ◽  
Stellar Proper Motions

scholarly journals The Luyten – Control Data Stellar Proper Motion Measuring Machine

1970 ◽  
Vol 7 ◽  
pp. 5-25
Author(s):  
James Newcomb
Keyword(s):  
Proper Motion ◽  
Time Scale ◽  
Proper Motions ◽  
Control Data ◽  
Stellar Proper Motions ◽  
Measurement Function ◽  
Measuring Machine ◽  
Motion Measurements

The discovery and measurement of stellar proper motions has always been associated with machines: for proper motion measurements involve four activities: observation, recording, comparison and measurement. Participation by the astronomer in these activities has step by step been replaced partically or wholly by machines. First the observation and recording functions changed from visual to photographic – with the fine guiding done by the astronomer; then the comparison by the blink microscope and the measurement by visually operated measuring machines. On a comparative time scale, the next step – automation of the comparison and measurement function – has been much money, time, and effort away from the previous steps, but as this presentation and other presentations at this conference will show, machines of varying degrees of automation and astronomer participation are now in operation.

scholarly journals Proper Motions With Respect to the Extragalactic Reference Frame

1990 ◽  
Vol 141 ◽  
pp. 407-417
Author(s):  
A. R. Klemola
Keyword(s):  
Reference Frame ◽  
Proper Motion ◽  
Milky Way ◽  
Proper Motions ◽  
Stellar Proper Motions

The Lick proper motion program, one of several using galaxies as a reference frame, is summarized with a statement of work accomplished for the non-Milky Way sky. The problem of identifying relatively transparent regions at low galactic latitudes is discussed, with tabular results presented for 41 windows from the literature having observable galaxies. These fields may be helpful for attaching stellar proper motions directly to the extragalactic frame.

THE EARLY GREAT DEBATE: A COMMENT ON IBN AL-HAYTHAM‘S WORK ON THE LOCATION OF THE MILKY WAY WITH RESPECT TO THE EARTH

2018 ◽  
Vol 28 (1) ◽  
pp. 1-30 ◽  
Author(s):  
Andreas Eckart
Keyword(s):  
Milky Way ◽  
Last Millennium ◽  
The Moon ◽  
Proper Motions ◽  
Stellar Proper Motions ◽  
The Earth ◽  
Great Debate ◽  
The Galaxy ◽  
Early Translation ◽  
Critical Translation

AbstractAt the very beginning of the last millennium Ibn al-Haytham greatly contributed to the investigation of the Milky Way. Here, the only three currently known versions of his work on the location of the Milky Way are compared to each other and discussed. A comparison of the texts and an early translation into German by E. Wiedemann in 1906 reveals several differences that triggered a new critical translation of the passed down text. We give detailed comments on the work and check the validity of Ibn al-Haytham's arguments. We also discuss his work in the framework of the ‘Great Debate’ on the Milky Way that took place around 1920, more than a decade after Wiedemann's translation. We find that Ibn al-Haytham's work is certainly at the peak of the unaided-eye era of the Milky Way's discovery. Through his own argumentation and in comparison to Ptolemy's observations Ibn al-Haytham clearly identifies the Galaxy as an extraterrestrial body that is not part of the atmosphere but much further away than the Moon. With some of his statements on the stellar positions passed down by Ptolemy, Ibn al-Haytham also anticipates the concept of stellar proper motions.

Relative proper motions in the region of the open cluster NGC 1664.

1973 ◽  
Vol 78 ◽  
pp. 53 ◽  
Author(s):  
S. J. Kerridge ◽  
R. M. Nelson ◽  
W. S. Mesrobian
Keyword(s):  
Open Cluster ◽  
Proper Motions

Proper motions of stars in the open cluster M 37.

1966 ◽  
Vol 71 ◽  
pp. 736 ◽  
Author(s):  
A. R. Upgren
Keyword(s):  
Open Cluster ◽  
Proper Motions

scholarly journals The dynamics of an extremely young cluster probed for the first time

2009 ◽  
Vol 5 (S266) ◽  
pp. 386-389
Author(s):  
Christine Ducourant ◽  
Sylvain Bontemps ◽  
Didier Despois ◽  
Philippe André ◽  
Ramachrisna Teixeira ◽  
...  
Keyword(s):  
Velocity Field ◽  
Proper Motion ◽  
Velocity Dispersion ◽  
Open Cluster ◽  
Extended Period ◽  
Early Evolution ◽  
Proper Motions ◽  
Crucial Importance ◽  
Cluster Systems ◽  
First Time

AbstractWe present a proper-motion program that we have developed at ESO to measure, for the first time, proper motions of members of the nearby (125 pc), very young (4 × 105 yr) infrared ρ Ophiuchi cluster. Repeated imaging over an extended period will allow us to measure the global proper motion of the cluster and its velocity dispersion and will provide access to the ~ 1 km s−1 velocities for objects as faint as K = 15.7 mag. Access to the velocity field of such an extremely young cluster is of crucial importance to investigate the origin and early evolution of open cluster systems.

scholarly journals The extended main-sequence turn-off of the Milky Way open cluster Collinder 347

2019 ◽  
Vol 490 (2) ◽  
pp. 2414-2420 ◽  
Author(s):  
Andrés E Piatti ◽  
Charles Bonatto
Keyword(s):  
Main Sequence ◽  
Milky Way ◽  
Open Cluster ◽  
Age Difference ◽  
Proper Motions ◽  
Gaussian Distributions ◽  
Young Object ◽  
Magnitude Diagram ◽  
Chemical Content ◽  
Gaia Dr2

ABSTRACT We made use of the Gaia DR2 archive to comprehensively study the Milky Way open cluster Collinder 347, known until now as a very young object of solar metal content. However, the G versus GBP − GRP colour–magnitude diagram (CMD) of bonafide probable cluster members, selected on the basis of individual stellar proper motions, their spatial distribution, and placement in the CMD, reveals the existence of a Hyades-like age open cluster (log(t /yr) = 8.8) of moderately metal-poor chemical content ([Fe/H]  = −0.4 dex), with a present-day mass of 3.3 × 103 M⊙. The cluster exhibits an extended main-sequence turn-off (eMSTO) of nearly 500 Myr, while that computed assuming Gaussian distributions from photometric errors, stellar binarity, rotation, and metallicity spread yields an eMSTO of ∼340 Myr. Such an age difference points to the existence within the cluster of stellar populations with different ages.

scholarly journals Stellar population of Sco OB2 revealed by Gaia DR2 data

2019 ◽  
Vol 623 ◽  
pp. A112 ◽  
Author(s):  
F. Damiani ◽  
L. Prisinzano ◽  
I. Pillitteri ◽  
G. Micela ◽  
S. Sciortino
Keyword(s):  
Stellar Population ◽  
Main Sequence ◽  
Open Cluster ◽  
Proper Motions ◽  
Lower Mass ◽  
Global Pattern ◽  
Field Star ◽  
Photometric Measurements ◽  
Stellar Masses ◽  
Gaia Dr2

Context. The Sco OB2 association is the nearest OB association, extending over approximately 2000 square degrees on the sky. Only its brightest and most massive members are already known (from HIPPARCOS) across its entire size, while studies of its lower mass population refer only to small portions of its extent. Aims. In this work we exploit the capabilities of Gaia DR2 measurements to search for Sco OB2 members across its entire size and down to the lowest stellar masses. Methods. We used both Gaia astrometric (proper motions and parallaxes) and photometric measurements (integrated photometry and colors) to select association members, using minimal assumptions derived mostly from the HIPPARCOS studies. Gaia resolves small details in both the kinematics of individual Sco OB2 subgroups and their distribution with distance from the Sun. We developed methods to explore the 3D kinematics of a stellar population covering large sky areas. Results. We find nearly 11 000 pre-main-sequence (PMS) members of Sco OB2 (with less than 3% field-star contamination), plus ∼3600 main-sequence (MS) candidate members with a larger (10–30%) field-star contamination. A higher confidence subsample of ∼9200 PMS (and ∼1340 MS) members is also selected (<1% contamination for the PMS), however this group is affected by larger (∼15%) incompleteness. We separately classify stars in compact and diffuse populations. Most members belong to one of several kinematically distinct diffuse populations, whose ensemble clearly outlines the shape of the entire association. Upper Sco is the densest region of Sco OB2. It is characterized by a complex spatial and kinematical structure and has no global pattern of motion. Other dense subclusters are found in Lower Centaurus-Crux and in Upper Centaurus-Lupus; the richest example of the latter, which has been recently identified, is coincident with the group near V1062 Sco. Most of the clustered stars appear to be younger than the diffuse PMS population, suggesting star formation in small groups that rapidly disperse and are diluted, reaching space densities lower than field stars while keeping memory of their original kinematics. We also find that the open cluster IC 2602 has a similar dynamics to Sco OB2, and its PMS members are currently evaporating and forming a diffuse (size ∼10°) halo around its double-peaked core.

scholarly journals Proper Motion Survey in the Pleiades

1995 ◽  
Vol 148 ◽  
pp. 228-231
Author(s):  
J. Souchay ◽  
E. Schilbach
Keyword(s):  
Proper Motion ◽  
Open Cluster ◽  
Photometric Data ◽  
Proper Motions ◽  
Total Field

AbstractAs a first step of our open cluster programme a catalogue of proper motions and photographic U, B, V, R magnitudes for stars up to 18 mag within a region centered near Alcyone is presented. The catalogue is based on MAMA measurements of plates taken with Tautenburg and OCA (CERGA) Schmidt telescopes. The photometric survey includes ca. 65000 stars and covers a total field of about 25 square degrees. Proper motions have been obtained for ca. 40000 stars within a central 17 square degree region of this field. For the majority of stars in the survey an accuracy of 0.08 mag and 2 mas/year has been estimated for photometric data and proper motions, respectively. The results of the determination of the Pleiades membership up to 18th magnitude is presented.

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